adsabs/AstroCLIMB huggingface dataset:
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption:  CASI-3D prediction for previously identified outflows in Ophiuchus (upper left), Taurus (upper right), Perseus (lower left), and Orion (lower right). Left: integrated 12CO emission. Middle: outflow emission predicted by CASI-3D. Blue and red contours indicate the blue- and redshifted lobes. Right: inclination angle predicted by CASI-3D across the outflows. The effective outflow inclination angles are 23° (upper left), 36° (upper right), 48° (lower left), and 40° (lower right). The red stars indicate the locations of YSOs (Gutermuth et al. 2009; Rebull et al. 2010; Pokhrel et al. 2020).
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Stacked probability distribution functions (PDF, top panel) and cumulative distribution functions (CDF, bottom panel) of the outflow inclination angles for the sources in the four regions.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Relation between the CASI-3D predicted outflow inclination angles and the true inclination angles for synthetic outflows. The error bars indicate the uncertainty of the inferred inclination angle for synthetic outflows with different physical and chemical conditions.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Same as Figure 1, but for Perseus.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Same as Figure 1, but for Taurus.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: CO, stellar, and Hα velocity maps for each galaxy. The MaNGA Plate-IFU identifier is in the top left of the CO velocity map, boxed in magenta for cPSB galaxies and orange for rPSB galaxies. The ALMA and MaNGA beams are represented by the yellow ellipse in the bottom left. The CO velocity map is shown where we have CO S/N > 3. The stellar velocity and Hα maps are only shown for spaxels with an S/N of 5 or an Hα S/N of 3. We fit each velocity map and plot the rotational PA in green for maps with reliable PA fits, with shaded 3σ uncertainties.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Scan technique used to observe M 104 with PACS. Each square is a position of the array on the sky with respect to the center of the galaxy. The scan has been repeated twice in opposite directions (blue and red squares). The numbers refer to the number of the slice used in the bottom panel figure, which shows the signal normalized to the median signal for all the 16 spexels in spaxel 2. The two different tonalities of green and blue indicate the two wavelength ranges observed in each position of the scan. In particular, the green slices are on-target positions while the blue ones are off-target positions (scan blocks 1, 13, and 25). The red line shows the fit of the transient behavior of the response. Note that the same position observed at the beginning (2) and end (33) of the observation has a variation of 15% in the response of the detectors, while the flux in the off-target positions varies by 20%.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: CO(1–0) spectra and integrated intensity contours for the 13 PSB galaxies in our sample. The spectra is spatially integrated over 1.5R  e . The shaded region shows the spectral integration bounds for the intensity maps. The MaNGA Plate-IFU identifier is boxed in purple for cPSBs galaxies and orange for rPSB galaxies. The CO moment 0 contours correspond to S/N values of 3, 4, 5, 8, 10, 15, and 30, and are plotted over the SDSS 3-color image. The 1σ noise levels for each galaxy are given in Table 1. The red plus denotes the optical center of the galaxy, and the red dashed line denotes the r-band effective radius from the NSA. The yellow circle in the lower left denotes the ALMA beam size.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: The fraction of total CO line flux within the 3σ beam size, f core, and the physical resolution of the 2.″5 CO beam for our cPSB galaxies in purple, rPSB galaxies in orange, and ALMaQUEST star-forming galaxies in blue. All galaxies plotted were imaged with the same 2.″5 circular beam. Our PSB galaxies tend to have higher core fractions and thus more centrally concentrated CO emission even at similar physical resolutions.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: Left: stellar mass and redshift diagram of our sample of cPSB and rPSB galaxies, ALMaQUEST star-forming galaxies, and the parent MaNGA DR15 sample as gray contours. We use stellar masses from Pace et al. (2019), and see that the majority of our PSB sample has lower masses than the ALMaQUEST star-forming sample. Right: color–magnitude diagram with the same galaxies plotted. Magnitudes are from the NSA. Error bars are present for all points but may be smaller than the marker size. Our cPSB galaxies tend to be redder than the star-forming sample while our rPSB galaxies have similar colors.
Paper: Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Authors: Justin Atsushi Otter, Kate Rowlands, Katherine Alatalo, Ho-Hin Leung, Vivienne Wild, Yuanze Luo, Andreea O. Petric, Elizaveta Sazonova, David V. Stark, Timothy Heckman, Timothy A. Davis, Sara Ellison, K. Decker French, William Baker, Asa F. L. Bluck, Lauranne Lanz, Lihwai Lin, Charles Liu, Carlos López Cobá, Karen L. Masters, Preethi Nair, Hsi-an Pan, 璽安 潘, Rogemar A. Riffel, Jillian M. Scudder, Adam Smercina, Freeke van de Voort, John R. Weaver
Figure caption: PCA classification results for our sample. Three images show the SDSS 3-color image for each galaxy, the excess Balmer absorption (PC2), and the PCA classification map. The MaNGA Plate-IFU number is above the first panel. The excess Balmer absorption is measured with the PCA method from Rowlands et al. (2018), where positive values (in teal) indicate PSB regions. The length of the black rectangle in the lower right shows the spatial scale of 1 kpc. The green ellipse in the bottom left shows the 2.″5 MaNGA average seeing. Finally, in the PCA classification map, PSB spaxels are magenta, SF spaxels are blue, GV spaxels are green, and quiescent spaxels are light red. The top-left text states whether the galaxy is classified as a cPSB or rPSB galaxy. The purple hexagons show the MaNGA IFU coverage.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Effect of transient corrections on a single pixel: spaxel 2, spexel 6. The original signal normalized to the telescope background (top panel) is fitted with a transient model (red line). The determined correction factor for the long term transient is shown in the middle panel. Additional corrections for short term transients caused by cosmic rays hitting the detector can be seen as spikes in this curve. These are corrected using the HIPE pipeline, leaving only the flux variations along the scan at the end of the process (bottom panel).
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: The transient at the beginning of each science block. The color code is as in Figure A1. On the top, the first estimates of the two science-block transients are obtained by fitting the last science blocks of all the 16 spexels of spaxel 2. On the bottom, the model is refined for the single spexel 6 of spaxel 2, using most of the science blocks of the observation, corrected for the long-term transient.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: 10 GHz total-intensity distribution of SNTF1 (G0.30-0.26). This image has a beam size of 4.″7 × 1.″8 and an rms noise level of ∼60 μJy beam−1.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: 6 GHz total-intensity distribution of SNTF3 (G359.69-0.41). This image has a beam size of 4.″5 × 2.″0 with an rms noise level of ∼42 μJy beam−1. Key features discussed in the text are labeled in the figure.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: Zoomed-in view of SNTF1 (G0.30-0.26) at 6 GHz. The beam size and rms noise level are the same as in Figure 2.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: Zoomed-in 6 GHz view of the Wishbone (G359.69-0.52). The beam size and rms noise level are the same as in Figure 9.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: 6 GHz total-intensity distribution of SNTF2 (G0.15–0.20). This image has a beam size of 4.″7 × 2.″1 and an rms noise level of ∼200 μJy beam−1. Key features are labeled in the figure.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: 10 GHz total-intensity distribution of SNTF2 (G0.15-0.20). This image has a beam size of 4.″6 × 2.″1 and an rms noise level of ∼20 μJy beam−1.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: Zoomed-in view of the Quill filament (G0.17-0.39) at 10 GHz. The beam size and rms noise level are the same as in Figure 6. The contrast in this image has been adjusted to emphasize the emission from the Quill.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: Zoomed-in view of the Quill filament (G0.17-0.39) at 6 GHz. The beam size and rms noise level are the same as in Figure 5. The contrast in this image has been adjusted to emphasize the emission from the Quill.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: Zoomed-in 6 GHz view of SNTF3 (G359.69-0.41). The beam size and rms noise level are the same as in Figure 9.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Mosaic of dust optical depth τ at 1 THz for 13 fields in the Taurus molecular cloud complex, embedded in the optical depth map from the Planck dust model. The companion mosaic of dust temperature T is in Figure 3.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Mosaic of dust temperature T, companion to mosaic of optical depth τ in Figure 2.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Histogram of the median β for individual HGBS fields.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: correlation of τ HGBS   (Pezzuto et al. 2021) with our τ HOTT  for Perseus E with a linear fit. Middle: correlation of T HGBS with our T HOTT. The line was fit with respect to the median of T HOTT (x − m  x ). Right: correlation of a predicted T (Section 12.1.2) with T HGBS.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Top: JDM of the brightest area of W3 at 250 μm from images taken at different values of POSANGLE. Bottom: simulation using only four appropriately placed and scaled bright point sources and the SPIRE beam map.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: ratio of τ HGBS  and τ HOTT,2 maps. Right: difference of T HGBS and T HOTT,2 maps. The τ HOTT,2 and T HOTT,2 are from the run where we generated HOTT maps using β = 2 and similar intensity errors as HGBS.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Normalized distribution functions of ﹩\mathrm{log}({\chi }^{2})﹩ for the Orion A-C field from HOTT (left) and HP2 (right). The theoretical curve for HP2 is for k = 3 degrees of freedom, because 100 μm data were used in the SED fits.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Like Figure 22, but comparing for HP2 maps of Perseus E (Zari et al. 2016) to HOTT. Right: when solving for the predicted T, we used the β map provided by HP2.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: ratio of τ HP2 and τ HOTT maps. Right: difference of T HP2 and T HOTT maps.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Ratio of τ HGBS   and τ HOTT,m maps, where τ HOTT,m is the τ HOTT  map modified using the fit from the left panel of Figure 22.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: ratio of τ HGBS  and τ HOTT  maps. Right: difference of T HGBS and T HOTT maps.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Normalized distribution functions of ﹩\mathrm{log}({\chi }^{2})﹩ for the Perseus E field from HOTT (left, as in Figure 14) and HP2 (right).
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: The evolution of the IR spectrum of the nova in the (a) far red + J band, and (b) H and K bands. Obtained with the Aerospace VNIRIS spectrograph, the 2016 observation was acquired using the Aerospace Corporation’s 1 m reflector; all subsequent measurements used the Lick Shane 3 m telescope. Neutral CNO emission lines are notably strong immediately following outburst, with little evidence for higher ionization at later epochs.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: Chiron spectra of resolution 11 km s−1 show the evolution of Hβ over time. The flux in each plot is normalized to the continuum flux near −2000 km s−1. The line profile shows two clear components, one broad and the other narrow. Each dominate at different times, but both are always present. Only the narrow component clearly shows absorption, with its P Cygni profile indicating an expanding gas of order ≲100 km s−1. The dashed vertical line represents the median velocity of the profile, corresponding to a radial velocity of the inhomogeneous emitting gas of −90 km s−1.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: Chiron spectra of the O I λ7773 multiplet at high resolution of 11 km s−1. Resolved absorption from intervening gas is frequently present, but no narrow-emission component is detected at any time. As with the O I λ8446 line, broad emission is present for the early years following outburst, but fades into the continuum thereafter.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: Spectral evolution of V5856 Sgr in the visible over the 6 yr period between outburst and the present time (2022). Data were obtained from (a) Aerospace 1 m AEROTEL telescope with VNIRIS spectrograph at coudé focus, (b–e, g) CTIO/SMARTS + Chiron spectrograph, (f) Asiago 1.22 m telescope + B&C Cassegrain spectrograph.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: The Luckas ARAS spectrum of 2016 November 9 displayed the strongest absorption lines. We identify some of the stronger lines with low-ionization heavy elements, indicative of an expanding photosphere of gas, much of which likely originated on the secondary star. Line blending due to the low spectral resolution causes some of the identifications to be uncertain.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: Chiron spectra showing the evolution of [N II] λ5755. The individual spectra are plotted with respect to the normalized continuum flux, and show considerable variation in the strength of [N II] over time relative to the continuum, whose brightness has not varied significantly in the visible over the past 6 yr. The continuum brightness changes by a factor of more than 2 among the different dates, and the profile consists entirely of the broad-emission component.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: Chiron spectra of He I λ6678 showing its evolution. As in all plots in Figures 6–11, the flux is normalized to the continuum flux near −2000 km s−1. Compared to Hβ the λ6678 broad-emission component is less prominent relative to its narrow component.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: Chiron spectra of [O III] λ5007 at high resolution of 0.18 Å (11 km s−1). After the initial optically thick fireball stage, where permitted lines dominate the spectrum, the [O III] emission becomes prominent. The emission peak at 400 km s−1 at early epochs is due to He I l5015 emission.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: High-resolution Chiron spectra of the O I λ8446 line. The narrow component dominates the emission after 2 yr following the outburst.
Paper: Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: David Berardo, Julien de Wit
Figure caption: This figure shows two views of the surface of WASP-19 b. Points in black show the spherical planet that matches the observed transit depth, while points in red show the surface generated by fitting for an equipotential while also matching the observed transit depth. On the left we see a top-down view of the orbital plane. On the right we see the view along the line of sight between the centers of mass of the planet and star.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: We display all the binary detections made in the F435W filter, showing one image per detection. The top panel shows the 21 × 21 postage stamp cutout of the HST/ACS data, the middle panel shows our double-PSF model, and the bottom panel shows the residuals. Each binary is labeled with its Source # that corresponds to a 2MASS ID listed in Table 3 and the estimated separation is given at the bottom of each image. Sources are listed left to right and top to bottom in order of increasing orbital separation. The color bar shows the dynamic range of all the images in units of detector counts.